### Abstract

We compare three different statistical models for the equation of state (EOS) of stellar matter at subnuclear densities and temperatures (0.5-10 MeV) expected to occur during the collapse of massive stars and supernova explosions. The models introduce the distributions of various nuclear species in nuclear statistical equilibrium, but use somewhat different nuclear physics inputs. It is demonstrated that the basic thermodynamical quantities of stellar matter under these conditions are similar, except in the region of high densities and low temperatures. We demonstrate that mass and isotopic distributions have considerable differences related to the different assumptions of the models on properties of nuclei at these stellar conditions. Overall, the three models give similar trends, but the details reflect the uncertainties related to the modeling of medium effects, such as the temperature and density dependence of surface and bulk energies of heavy nuclei, and the nuclear shell structure effects. We discuss importance of new physics inputs for astrophysical calculations from experimental data obtained in intermediate energy heavy-ion collisions, in particular, the similarities of the conditions reached during supernova explosions and multifragmentation reactions.

Original language | English |
---|---|

Pages (from-to) | 13-54 |

Number of pages | 42 |

Journal | Nuclear Physics A |

Volume | 907 |

DOIs | |

Publication status | Published - 2013 Jun 3 |

### Fingerprint

### Keywords

- Nuclear astrophysics

### ASJC Scopus subject areas

- Nuclear and High Energy Physics

### Cite this

*Nuclear Physics A*,

*907*, 13-54. https://doi.org/10.1016/j.nuclphysa.2013.03.010

**A comparative study of statistical models for nuclear equation of state of stellar matter.** / Buyukcizmeci, N.; Botvina, A. S.; Mishustin, I. N.; Ogul, R.; Hempel, M.; Schaffner-Bielich, J.; Thielemann, F. K.; Furusawa, S.; Sumiyoshi, K.; Yamada, Shoichi; Suzuki, H.

Research output: Contribution to journal › Article

*Nuclear Physics A*, vol. 907, pp. 13-54. https://doi.org/10.1016/j.nuclphysa.2013.03.010

}

TY - JOUR

T1 - A comparative study of statistical models for nuclear equation of state of stellar matter

AU - Buyukcizmeci, N.

AU - Botvina, A. S.

AU - Mishustin, I. N.

AU - Ogul, R.

AU - Hempel, M.

AU - Schaffner-Bielich, J.

AU - Thielemann, F. K.

AU - Furusawa, S.

AU - Sumiyoshi, K.

AU - Yamada, Shoichi

AU - Suzuki, H.

PY - 2013/6/3

Y1 - 2013/6/3

N2 - We compare three different statistical models for the equation of state (EOS) of stellar matter at subnuclear densities and temperatures (0.5-10 MeV) expected to occur during the collapse of massive stars and supernova explosions. The models introduce the distributions of various nuclear species in nuclear statistical equilibrium, but use somewhat different nuclear physics inputs. It is demonstrated that the basic thermodynamical quantities of stellar matter under these conditions are similar, except in the region of high densities and low temperatures. We demonstrate that mass and isotopic distributions have considerable differences related to the different assumptions of the models on properties of nuclei at these stellar conditions. Overall, the three models give similar trends, but the details reflect the uncertainties related to the modeling of medium effects, such as the temperature and density dependence of surface and bulk energies of heavy nuclei, and the nuclear shell structure effects. We discuss importance of new physics inputs for astrophysical calculations from experimental data obtained in intermediate energy heavy-ion collisions, in particular, the similarities of the conditions reached during supernova explosions and multifragmentation reactions.

AB - We compare three different statistical models for the equation of state (EOS) of stellar matter at subnuclear densities and temperatures (0.5-10 MeV) expected to occur during the collapse of massive stars and supernova explosions. The models introduce the distributions of various nuclear species in nuclear statistical equilibrium, but use somewhat different nuclear physics inputs. It is demonstrated that the basic thermodynamical quantities of stellar matter under these conditions are similar, except in the region of high densities and low temperatures. We demonstrate that mass and isotopic distributions have considerable differences related to the different assumptions of the models on properties of nuclei at these stellar conditions. Overall, the three models give similar trends, but the details reflect the uncertainties related to the modeling of medium effects, such as the temperature and density dependence of surface and bulk energies of heavy nuclei, and the nuclear shell structure effects. We discuss importance of new physics inputs for astrophysical calculations from experimental data obtained in intermediate energy heavy-ion collisions, in particular, the similarities of the conditions reached during supernova explosions and multifragmentation reactions.

KW - Nuclear astrophysics

UR - http://www.scopus.com/inward/record.url?scp=84875764705&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84875764705&partnerID=8YFLogxK

U2 - 10.1016/j.nuclphysa.2013.03.010

DO - 10.1016/j.nuclphysa.2013.03.010

M3 - Article

AN - SCOPUS:84875764705

VL - 907

SP - 13

EP - 54

JO - Nuclear Physics A

JF - Nuclear Physics A

SN - 0375-9474

ER -